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The redshift drift, the change of cosmological redshift with time, is adirect consequence of the expansion of the Universe. Thus the measurement ofthe cosmological redshift drift will offer a direct test of our models ofcosmology. The magnitude of the effect is very small, i.e. the spectral shiftis of order of $10^{-10} - 10^{-9}$ over the period of a decade, but the nextgeneration facilities such as ELT and SKA will be able to directly detect theexpansion of our Universe by the year 2040. In this paper we focus ondetectebility of this effect, including strategies of overcoming the kinematiccontamination of the cosmological signal. We also show that the redshift driftdirectly impacts the change of flux. Thus apart from the redshift drift,measurements of the flux drift will provide an additional tool of detecting theexpansion of the universe, including its acceleration. We discuss thestrategies of detecting the flux drift and show that by including the fluxdrift signal to the redshift drift signal we boost the chances of a directdetection of the expansion of the Universe. We show that if only the stabilityof flux is at the level of $\Delta F/F \sim 10^{-6}$ then the SKA1-mid Arrayshould be able to detect these effects, before the ETL and the full SKA. Thus,by including the flux drift into the SKA1-mid Array's analysis pipeline, wecould be able to provide by mid-2030s a direct evidence of the expansion of theuniverse including its accelerating phase.

Direct detection of the cosmic expansion: the redshift drift and the flux drift